By Frank J. Low (auth.), Giovanni G. Fazio (eds.)
The Symposium on Infrared and Submillimeter Astronomy used to be held in Philadelphia, Pennsylvania, america, on June 8-10, 1976, as an task linked to the 19th Plenary assembly of the Committee on area examine (CaSPAR). The Symposium used to be backed together via CaSPAR, the foreign Astronomical Union (IAU) and the foreign Union of Radio technology CURSI). caSPAR is an interdisciplinary clinical association, verified via the overseas Council of clinical Unions in 1958, to, within the phrases of its constitution, "provide the area clinical neighborhood with the capability wherein it could possibly make the most the probabilities of satellites and area probes of all types for medical reasons and trade the ensuing facts on a co operative basis." the aim of this actual CaSPAR Sympo sium used to be to give new leads to infrared and submillimeter astronomy got through observations on plane, excessive altitude balloons, rockets, satellites, and house probes. issues dis stubborn incorporated the solar, the sun procedure, galactic and additional galactic gadgets in addition to the cosmic history radiation. Instrumentation for observations in infrared and submillimeter astronomy used to be additionally mentioned, with specific emphasis on destiny courses from area observatories.
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Extra info for Infrared and Submillimeter Astronomy: Proceedings of a Symposium Held in Philadelphia, Penn., U.S.A., June 8–10, 1976
341. , in press. J. 1976, ~. ~. (Letters), in press. D. Q. 1974, Astr. Y. P. 1976, ~. , ~, 469. J. (Letters), 205, L21. J. 1973, AFCRL-TR-037l. H. 1976, (Letters), in press. ~. J. M. 1975, Bull. , 433. M. T. 1974, ~. ~. (Letters), 189, L27. T. 1975, Bull. , l, 429. Racine, R. 1968, ! , 588. Neugebauer, G. B. 1969, NASA SP-3047. G. 1975, ~. J. (Letters), 198, L129. W. P. 1974, A. , li, 797. G. D. 1975, AFCRL-TR-75-0373. G. 1975, ~. , 202, 407. , and Palmer, D. 1976, ~. ~. (Letters), 205, LIS.
8 49 J 10 " 12 13 " (I'm) Fig. 3. lm" band observed in the Trapezium region (solid line) is compared with that computed for the lunar silicate No. 14321 (dashed line). The opacities are normalized to the peak value. lm are indicated (dotted curves). component which dominates the UV absorption and the FIR emission, has a high FIR and SMI absorption efficiency, and has a relatively high abundance and large size. ). g. Gillett and Forrest, 1973; Soifer et al. 1976). lm attenuated by an absorption band with the same profile (Aitken and Jones, 1973; Gillett et al.
1976) observed on two different occasions, a third varied by a factor of two or more. The time difference between the two sets of observations was one year. This behavior is reminiscent of the variability observed by Strecker and Ney (1974) among many of the new stars that were found in the Twp Micron Sky Survey. Taken together, these data suggest that most of the new AFCRL sources are late-type giants and super-giants similar to the sources of high I-K index discovered in the Two Micron Sky Survey (Neugebauer and Leighton, 1969).